The optical reference information files have been updated to reflect the Phase A payload design. This is the design that is baselined for the upcoming System Requirements Review and Baseline Design Review.
» WFIRST Observatory Reference Information (.pptx) A compendium of basic information on the WFIRST Observatory, as of July 31, 2017.
» WFIRST Wide-Field Instrument Reference Information (.pptx) A compendium of basic reference information on the WFIRST Wide-Field Instrument, August 1, 2017
» WFIRST SRR: Data from WFC Model (.xlsm)
Point-spread functions for the WFIRST Wide-Field Instrument (aka 'Wide Field Channel') can be computed at any wavelength and at any position in the field of view, given knowledge of the pupil function. The file gives Zernike decompositions of the wavefront error needed to perform this calculation; links to the pupil masks are given below. In addition to imaging mode, the Zernike coefficients are provided for the grism Wide-Field Spectroscopy Mode (WSM) in first order, and for a single field position in 0th and 2nd order. This file also provides a fit to distortions in WFI imaging mode (WIM), a mapping of WIM detector positions onto the sky, WFI SCA positions in the focal plane, etc.
» Explanation of Zernike coefficients (.docx) Contains descriptions of the columns in the preceding file.
» WFIRST (SRR Design) Exit Pupil Masks for the Wide Field Instrument (.pptx) This describes the orientation of the pupils, and includes other relevant information.
» WFIRST MCR WFI Pupils (.pptx) Orientation of the pupils, and includes other relevant information.
» Grism Mode SCA Projected Fields (.xlsx) This spreadsheet provides a calculator for each SCA giving the mapping in both directions between sky angle and wavelength to detector position.
» WFIRST MCR WSM Dispersion Fits (.xlsx) This spreadsheet provides a calculator for each SCA giving the mapping in both directions between sky angle and wavelength to detector position.
» WFIRST Wide-Field Instrument Transmission (.xlsx) Contains information for calculating the Effective area as a function of wavelength for each observing mode of the Wide-Field Instrument.